{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:PDJFWIMQDYLAIYAEGZPLY2QMYN","short_pith_number":"pith:PDJFWIMQ","schema_version":"1.0","canonical_sha256":"78d25b21901e16046004365ebc6a0cc35f4dfc3dfeb0011debb0ddf45b2380e9","source":{"kind":"arxiv","id":"2401.15180","version":2},"attestation_state":"computed","paper":{"title":"Neutron star kick driven by asymmetric fast-neutrino flavor conversion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Hiroki Nagakura, Kohsuke Sumiyoshi","submitted_at":"2024-01-26T19:59:16Z","abstract_excerpt":"Multi-dimensional nature of core-collapse supernova (CCSN) leads to asymmetric matter ejection and neutrino emission, that potentially accounts for the origin of neutron star (NS) kick. Asymmetric neutrino radiation fields are, in general, accompanied by large-scale inhomogeneous fluid distributions, in particular for electron-fraction ($Y_e$) distributions. Recently, it has also been revealed that lower $Y_e$ environments in proto-neutron star envelope can offer preferable conditions for collective neutrino oscillations. In this paper, we show that a dipole asymmetry of fast neutrino-flavor c"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2401.15180","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-01-26T19:59:16Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"a885808a9b8da8cd8bd5276d46e993bf691f92d03fa68de71588d94cbf9615c7","abstract_canon_sha256":"a6a121253b949a51c33979c5a3b8676686a9af8156a0fc3f4587d3cfaa9f8a4c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:11:57.308290Z","signature_b64":"j5pkAhpt6rnw7N/TH7Kw8C255Ab3nEAPm/pMcX9pBOkrwmmiqJoosBVY22JlJhYQA+LRPgxo7BW02OoYu5MtBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"78d25b21901e16046004365ebc6a0cc35f4dfc3dfeb0011debb0ddf45b2380e9","last_reissued_at":"2026-07-05T08:11:57.307811Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:11:57.307811Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Neutron star kick driven by asymmetric fast-neutrino flavor conversion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Hiroki Nagakura, Kohsuke Sumiyoshi","submitted_at":"2024-01-26T19:59:16Z","abstract_excerpt":"Multi-dimensional nature of core-collapse supernova (CCSN) leads to asymmetric matter ejection and neutrino emission, that potentially accounts for the origin of neutron star (NS) kick. Asymmetric neutrino radiation fields are, in general, accompanied by large-scale inhomogeneous fluid distributions, in particular for electron-fraction ($Y_e$) distributions. Recently, it has also been revealed that lower $Y_e$ environments in proto-neutron star envelope can offer preferable conditions for collective neutrino oscillations. In this paper, we show that a dipole asymmetry of fast neutrino-flavor c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2401.15180","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2401.15180/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2401.15180","created_at":"2026-07-05T08:11:57.307868+00:00"},{"alias_kind":"arxiv_version","alias_value":"2401.15180v2","created_at":"2026-07-05T08:11:57.307868+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2401.15180","created_at":"2026-07-05T08:11:57.307868+00:00"},{"alias_kind":"pith_short_12","alias_value":"PDJFWIMQDYLA","created_at":"2026-07-05T08:11:57.307868+00:00"},{"alias_kind":"pith_short_16","alias_value":"PDJFWIMQDYLAIYAE","created_at":"2026-07-05T08:11:57.307868+00:00"},{"alias_kind":"pith_short_8","alias_value":"PDJFWIMQ","created_at":"2026-07-05T08:11:57.307868+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.13617","citing_title":"Fast Neutrino-Flavor Conversion with Attenuation and Global Lepton Gradient","ref_index":15,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN","json":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN.json","graph_json":"https://pith.science/api/pith-number/PDJFWIMQDYLAIYAEGZPLY2QMYN/graph.json","events_json":"https://pith.science/api/pith-number/PDJFWIMQDYLAIYAEGZPLY2QMYN/events.json","paper":"https://pith.science/paper/PDJFWIMQ"},"agent_actions":{"view_html":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN","download_json":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN.json","view_paper":"https://pith.science/paper/PDJFWIMQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2401.15180&json=true","fetch_graph":"https://pith.science/api/pith-number/PDJFWIMQDYLAIYAEGZPLY2QMYN/graph.json","fetch_events":"https://pith.science/api/pith-number/PDJFWIMQDYLAIYAEGZPLY2QMYN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN/action/storage_attestation","attest_author":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN/action/author_attestation","sign_citation":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN/action/citation_signature","submit_replication":"https://pith.science/pith/PDJFWIMQDYLAIYAEGZPLY2QMYN/action/replication_record"}},"created_at":"2026-07-05T08:11:57.307868+00:00","updated_at":"2026-07-05T08:11:57.307868+00:00"}